Speaker
Description
We investigate the ejection mechanism in a relativistic, magnetized, viscous, advective accretion flow around a rotating
black hole (BH) in presence of radiative cooling. Considering the accretion flow to be threaded by toroidal magnetic fields, we self-consistently solve the coupled governing equations that describe the accretion-ejection scenario in terms of the dissipation parameters, namely viscosity ($\alpha$), accretion rate ($\dot m$) and plasma$\beta$. With this, we compute the outflow rate ($R_{\dot m}$) defined as the ratio of outflow to inflow mass flux and find that $R_{\dot m}$ increases as the magnetic activity inside the disk is increased. Further, we observe that nearly $30\%$ ($24\%$) accreted matter is ejected from a magnetized disc (inner edge plasma-$\beta \sim 30$) around a rapidly (weakly) rotating black hole of spin $a_{\rm k} = 0.99$ ($0.0$). Finally, we discuss the astrophysical implications of this formalism in explaining the jet kinetic power commonly observed in black holes systems.
| camelia_jana@iitg.ac.in | |
| Affiliation | IIT Guwahati |
